J/AJ/148/37ivo://CDS.VizieR/J/AJ/148/37doi:10.26093/cds/vizier.51480037CDSLee J.W.Kim S.-L.Hong K.Lee C.-U.Koo J.-R.2017-06-13T11:08:27Z2014-11-17T14:04:59ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.freclipsing-binary-starsWe present the physical properties of V404 Lyr exhibiting eclipse timing variations and multiperiodic pulsations from all historical data including the Kepler and SuperWASP observations. Detailed analyses of 2922 minimum epochs showed that the orbital period has varied through a combination of an upward-opening parabola and two sinusoidal variations, with periods of P_3_=649days and P_4_=2154days and semi-amplitudes of K_3_=193s and K_4_=49s, respectively. The secular period increase at a rate of +1.41x10^-7^days/yr could be interpreted as a combination of the secondary to primary mass transfer and angular momentum loss. The most reasonable explanation for both sinusoids is a pair of light-travel-time effects due to two circumbinary objects with projected masses of M_3_=0.47M_{sun}_ and M_4_=0.047M_{sun}_. The third-body parameters are consistent with those calculated using the Wilson-Devinney binary code. For the orbital inclinations i_4_>~43{deg}, the fourth component has a mass within the hydrogen-burning limit of ~0.07M_{sun}_, which implies that it is a brown dwarf. A satisfactory model for the Kepler light curves was obtained by applying a cool spot to the secondary component. The results demonstrate that the close eclipsing pair is in a semi-detached, but near-contact, configuration; the primary fills approximately 93% of its limiting lobe and is larger than the lobe-filling secondary. Multiple frequency analyses were applied to the light residuals after subtracting the synthetic eclipsing curve from the Kepler data. This revealed that the primary component of V404 Lyr is a {gamma} Dor type pulsating star, exhibiting seven pulsation frequencies in the range of 1.85-2.11/day with amplitudes of 1.38-5.72mmag and pulsation constants of 0.24-0.27days. The seven frequencies were clearly identified as high-order low-degree gravity-mode oscillations which might be excited through tidal interaction. Only eight eclipsing binaries have been known to contain {gamma} Dor pulsating components and, therefore, V404 Lyr will be an important test bed for investigating these rare and interesting objects.2014AJ....148...37Lhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/AJ/148/37CatalogResearchIsServedByTAP VizieR generic servicerelated-toB/gcvs : General Catalogue of Variable Stars (Samus+ 2007-2013)J/AJ/147/45 : Kepler mission. IV. Eclipse times for close binariesJ/AJ/142/160 : Kepler Mission. II. 2165 eclipsing binaries (Slawson+, 2011)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/AJ/148/37https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/AJ/148/37http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/AJ/148/37https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/AJ/148/37https://vizier.iucaa.in/viz-bin/votable?-source=J/AJ/148/37http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/AJ/148/37GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapOpticaldefaultJ/AJ/148/37/table1SuperWASP (Wide Angle Search for Planets) and Kepler eclipse timings for V404 LyrrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintBJDBarycentric Julian Date (1)dtime.epoch;obsdoublee_BJDError in BJD (1)dstat.error;time.epoch;obsdoubleEpoch[-989/1966] Epoch (cycle) numbertime.epoch;meta.numberfloatO-C1Residual from Equation (1) ephemeris (2)dstat.fit.residual;time.epochdoubleO-C2Residual from Equation (2) ephemeris (3)dstat.fit.residual;time.epochdouble